A microlensing study of the accretion disc in the quasar MG 0414+0534

• Published in: Monthly notices of the Royal Astronomical Society Vol. 391; no. 4; pp. 1955 - 1960
• Main Authors: Bate, N. F., Floyd, D. J. E., Webster, R. L., Wyithe, J. S. B.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Publishing Ltd 21-12-2008; Wiley-Blackwell; Oxford University Press
• Subjects: accretion; accretion discs; Accretion disks; accretion, accretion discs; Astronomy; Earth, ocean, space; Exact sciences and technology; gravitational lensing; Quasars; quasars: individual: MG 0414+0534; gravitational lensing; accretion, accretion discs; quasars: individual: MG 0414+0534; Continuum; Quasars; Upper bound; Variability; Microlenses; Gravitational lensing; Models; Accretion disks; Power law; Multiple image
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2008.14020.x

Observations of gravitational microlensing in multiply imaged quasars currently provide the only direct probe of quasar emission region structure on submicroarcsecond scales. The analyses of microlensing variability are observationally expensive, requiring long-term monitoring of lensed systems. Here, we demonstrate a technique for constraining the size of the quasar continuum emission region as a function of wavelength using single-epoch multiband imaging. We have obtained images of the lensed quasar MG 0414+0534 in five wavelength bands using the Magellan 6.5-m Baade telescope at Las Campanas Observatory, Chile. These data, in combination with two existing epochs of Hubble Space Telescope data, are used to model the size of the continuum emission region σ as a power law in wavelength, σ∝λν. We place an upper limit on the Gaussian width of the r′-band emission region of 1.80 × 1016h−1/270 (〈M〉/M⊙)1/2cm, and constrain the power-law index to 0.77 ≤ν≤ 2.67 (95 per cent confidence range). These results can be used to constrain models of quasar accretion discs. As an example, we find that the accretion disc in MG 0414+0534 is statistically consistent with a Shakura–Sunyaev thin-disc model.